Evolution of twisted magnetic fields
Abstract
The magnetic field of the solar corona evolves quasistatically in response to slowly changing photospheric boundary conditions. The magnetic topology is preserved by the low resistivity of the solar atmosphere. It is shown that a magnetic flux coordinate system simplifies the problem of calculating field evolution with invariant topology. As an example, the equilibrium of a thin magnetic flux tube with small twist per unit length is calculated.
 Publication:

The Astrophysical Journal
 Pub Date:
 August 1985
 DOI:
 10.1086/163407
 Bibcode:
 1985ApJ...295..642Z
 Keywords:

 Magnetic Field Configurations;
 Magnetic Flux;
 Magnetohydrodynamic Stability;
 Photosphere;
 Solar Corona;
 Solar Magnetic Field;
 Cartesian Coordinates;
 Differential Equations;
 Euler Equations Of Motion;
 Integral Equations;
 Topology;
 Solar Physics